Dr
Vikram Dwarkadas
28/06/2011 09:35
I will review the evolution of SN shock waves in the surrounding medium, using analytic solutions and numerical simulations. I will discuss both white-dwarf and core-collapse SNe, the medium surrounding these SNe, and their evolution through various phases.
Dr
Nikos Prantzos
(IAP Paris)
28/06/2011 10:10
I explore the implications of a model in which cosmic rays
are accelerated by the forward shocks of supernovae exploding
within massive star winds, by using realistic stellar models
with mass loss and rotation. Using the same models, I
also show that the idea that the bulk of Galactic cosmic
rays are accelerated in superbubbles fails to reproduce
the key observable of GCR composition,...
Dr
Salavtore Orlando
(INAF osservatorio di Palermo)
28/06/2011 10:30
The thermal structure of the post-shock region of a young supernova remnant (SNR) is heavily affected by two main physical effects, namely the back-reaction of accelerated cosmic rays and the Rayleigh-Taylor instabilities developing at the contact discontinuity between the ejecta and the shocked interstellar medium (ISM). In this contribution, we investigate the role played by both physical...
Dr
Christian Farnier
(ISDC Geneva)
28/06/2011 11:20
One of the most outstanding stellar object in our Galaxy, eta Carinae, a colliding wind binary with the largest mass loss rate observed, presents a hard X-ray emission and is therefore a primary candidate to search for particle acceleration by probing its gamma-ray emission.
The detection of eta Carinae at high energy through analysis of Fermi/LAT data between 0.2 to 100 GeV was reported in...
Dr
Daria Kosenko
(Astronomical Institut Utrecht)
28/06/2011 11:40
We present numerical models for supernova remnant evolution, using a
new version of the hydrodynamical code SUPREMNA. We added cosmic ray
diffusion equation to the code scheme, employing two-fluid
approximation. We investigate the dynamics of the simulated supernova
remnants with different values of cosmic ray acceleration efficiency
and diffusion coefficient. We compare the...
